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X-Ray Timing of the Young Pulsar in 3C 58

Scott Ransom·Fernando Camilo·Victoria Kaspi·Patrick Slane·Bryan Gaensler·Eric Gotthelf·Stephen Murray
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Abstract

PSR J0205+6449 is a young pulsar in the Crab-like pulsar wind nebula 3C 58 which is thought to be a result of the historical supernova SN1181 CE. The 65.7-ms pulsar is the second most energetic of the known Galactic pulsars and has been shown to be remarkably cool for its age, implying non-standard cooling processes in the neutron star core. We report on RXTE timing observations taken during AO7 and supplemented by monthly radio observations of the pulsar made with the Green Bank Telescope (GBT). The total duration covered with the timing solutions is 450 days. We measure very high levels of timing noise from the source and find evidence for a ``giant'' glitch of magnitude Delta nu/nu ~ 1x10^-6 that occurred in 2002 October. We have also measured the phase-resolved spectra of the pulsations and find them to be surprisingly hard, with photon indices Gamma = 0.84 +0.06/-0.15 for the main pulse and Gamma = 1.0 +0.4/-0.3 for the interpulse assuming an absorbed power-law model.

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Scott Ransom, Fernando Camilo, Victoria Kaspi, Patrick Slane, Bryan Gaensler, Eric Gotthelf, Stephen Murray. 2004-01-08. X-Ray Timing of the Young Pulsar in 3C 58. https://doi.org/10.1063/1.1781054

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